All Figures

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{5321fig1.eps}\end{figure}$ Figure 1: Nearest Neighbor distribution in the VL1 sample: different symbols correspond to different angular regions. The average distance between nearest galaxies is $\langle \Lambda \rangle = 1.7$ Mpc/h. For reference the solid line represents the NN distribution for a Poisson configuration with the same $\langle \Lambda \rangle$ : the tails of this function decay more rapidly.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{5321fig2.eps}\end{figure}$ Figure 2: As Fig. 1 but for the VL2 samples. The average distance between galaxies is $\langle \Lambda \rangle = 1.3$ Mpc/h.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{5321fig3.eps}\end{figure}$ Figure 3: As Fig. 1 but for the VL3 samples. The average distance between nearest galaxies is $\langle \Lambda \rangle = 2.9$ Mpc/h.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{5321fig4.eps}\end{figure}$ Figure 4: As Fig. 1 but for the VL4 samples.The average distance between nearest galaxies is $\langle \Lambda \rangle = 6$ Mpc/h.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{5321fig5.eps}\end{figure}$ Figure 5: Differential number counts as a function of distance in the VL1 sample in different angular regions normalized to their own solid angle.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{5321fig6.eps}\end{figure}$ Figure 6: The same as Fig. 5 but for the VL2 samples.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{5321fig7.eps}\end{figure}$ Figure 7: The same as Fig. 5 but for the VL3 samples.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{5321fig8.eps}\end{figure}$ Figure 8: The same as Fig. 5 but for the VL4 samples.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{5321fig9.eps}\end{figure}$ Figure 9: Conditional density in spheres in the VL1 sample in the angular region R1, R2, R3. Here and in Figs. 10-12 we report, for each sample, a vertical line corresponding to the distance scale $R_{\rm c}$ discussed in Sect. 3.2 and shown in Table 4 (solid-line for R1, dotted-line for R2 and dashed-line for R3).
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{5321fig10.eps}\end{figure}$ Figure 10: As for Fig. 9 but for the VL2 samples.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{5321fig11.eps}\end{figure}$ Figure 11: As for Fig. 9 but for the VL3 samples.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{5321fig12.eps}\end{figure}$ Figure 12: As for Fig. 9 but for the VL4 samples.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{5321fig13.eps}\end{figure}$ Figure 13: Conditional density in spheres in the R1VL1 sample and in the 2 subsamples defined by the angular cut performed as discussed in the text. The lines labeled with $N_{\rm c}$ represent the behavior of the number of centers used in the average (Eq. (7)) arbitrarily normalized.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{5321fig14.eps}\end{figure}$ Figure 14: As Fig. 13 but for the R1VL2 sample.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{5321fig15.eps}\end{figure}$ Figure 15: As Fig. 13 but for the R1VL3 sample.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{5321fig16.eps}\end{figure}$ Figure 16: As Fig. 13 but for the R1VL4 sample.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{5321fig17.eps}\end{figure}$ Figure 17: Conditional density in spheres in the R1VL3 and R1VL4 samples, normalized to have the same amplitude at 1 Mpc/h. The large scale behavior (r> 30 Mpc/h) is different due to the effect of systematic fluctuations.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{5321fig18.eps}\end{figure}$ Figure 18: Conditional density for the four samples of points selected in the simulation: the original dark matter (DM) field, all "galaxies'' (ALL), blue galaxies (BLUE) and red galaxies (RED). The conditional density for dark matter particles (DM) has been normalized arbitrarily. The reference dashed-dotted line has a slope $\gamma =1.7$ . The dashed line with $\gamma =1$ , corresponding to the slope measured in the galaxy samples is also reported.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{5321fig19.eps}\end{figure}$ Figure 19: Nearest neighbors probability distribution for three point sets selected in the simulation (see discussion in the text): all "galaxies'' (ALL), blue galaxies (BLUE) and red galaxies (RED).
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{5321fig1.eps}\end{figure}$	Figure 1: Nearest Neighbor distribution in the VL1 sample: different symbols correspond to different angular regions. The average distance between nearest galaxies is $\langle \Lambda \rangle = 1.7$ Mpc/h. For reference the solid line represents the NN distribution for a Poisson configuration with the same $\langle \Lambda \rangle$ : the tails of this function decay more rapidly.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{5321fig2.eps}\end{figure}$	Figure 2: As Fig. 1 but for the VL2 samples. The average distance between galaxies is $\langle \Lambda \rangle = 1.3$ Mpc/h.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{5321fig3.eps}\end{figure}$	Figure 3: As Fig. 1 but for the VL3 samples. The average distance between nearest galaxies is $\langle \Lambda \rangle = 2.9$ Mpc/h.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{5321fig4.eps}\end{figure}$	Figure 4: As Fig. 1 but for the VL4 samples.The average distance between nearest galaxies is $\langle \Lambda \rangle = 6$ Mpc/h.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{5321fig5.eps}\end{figure}$	Figure 5: Differential number counts as a function of distance in the VL1 sample in different angular regions normalized to their own solid angle.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{5321fig6.eps}\end{figure}$	Figure 6: The same as Fig. 5 but for the VL2 samples.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{5321fig7.eps}\end{figure}$	Figure 7: The same as Fig. 5 but for the VL3 samples.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{5321fig8.eps}\end{figure}$	Figure 8: The same as Fig. 5 but for the VL4 samples.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{5321fig9.eps}\end{figure}$	Figure 9: Conditional density in spheres in the VL1 sample in the angular region R1, R2, R3. Here and in Figs. 10-12 we report, for each sample, a vertical line corresponding to the distance scale $R_{\rm c}$ discussed in Sect. 3.2 and shown in Table 4 (solid-line for R1, dotted-line for R2 and dashed-line for R3).
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{5321fig10.eps}\end{figure}$	Figure 10: As for Fig. 9 but for the VL2 samples.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{5321fig11.eps}\end{figure}$	Figure 11: As for Fig. 9 but for the VL3 samples.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{5321fig12.eps}\end{figure}$	Figure 12: As for Fig. 9 but for the VL4 samples.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{5321fig13.eps}\end{figure}$	Figure 13: Conditional density in spheres in the R1VL1 sample and in the 2 subsamples defined by the angular cut performed as discussed in the text. The lines labeled with $N_{\rm c}$ represent the behavior of the number of centers used in the average (Eq. (7)) arbitrarily normalized.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{5321fig14.eps}\end{figure}$	Figure 14: As Fig. 13 but for the R1VL2 sample.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{5321fig15.eps}\end{figure}$	Figure 15: As Fig. 13 but for the R1VL3 sample.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{5321fig16.eps}\end{figure}$	Figure 16: As Fig. 13 but for the R1VL4 sample.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{5321fig17.eps}\end{figure}$	Figure 17: Conditional density in spheres in the R1VL3 and R1VL4 samples, normalized to have the same amplitude at 1 Mpc/h. The large scale behavior (r> 30 Mpc/h) is different due to the effect of systematic fluctuations.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{5321fig19.eps}\end{figure}$	Figure 19: Nearest neighbors probability distribution for three point sets selected in the simulation (see discussion in the text): all "galaxies'' (ALL), blue galaxies (BLUE) and red galaxies (RED).
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